7,030 research outputs found
The affective notes of represented space as motors of emotional and sensorial response
The following essay proposes to investigate the perceptual and
emotional aspects related to the visualization of architectural images. The
field of research is limited to a well-defined category: figurative
representations as the photographic and digital images of contemporary
architecture. In particular, two types will be analysed: the un-built
architecture produced by Studio MIR and Bloomimages compared with the
photographed built architecture. Using figurative images as a tool of
reading, the aim of this work is to identify and classify three types of
affective spaces capable of generating a specific kind of perception,
producing a sensorial classification of atmosphere for architecture. The
study of the Psychology of Art, as well as Aesthetics and Neuroaesthetics
can be a valuable tool in understanding the phenomena of the present,
considering the marked pictoriality of these images. The application of the
analytic methodology, developed in these disciplines, can suggest a new
way of "looking" at the project, paying attention to the representation of the
atmospheres, which characterizes the experience of felt space
The Indirect Search for Dark Matter from the centre of the Galaxy with the Fermi LAT
Dark matter (DM) constitutes around a 25% of the Universe, while baryons only
a 4%. DM can be reasonably assumed to be made of particles, and many theories
(Super-symmetry, Universal Extra Dimensions, etc.) predict Weakly Interacting
Massive Particles (WIMPs) as natural DM candidates at the weak scale.
Self-annihilation (or decay) of WIMPs might produce secondary gamma-rays, via
hadronization or as final state radiation. Since its launch in the 2008, the
Large Area Telescope on-board of the Fermi gamma-ray Space Telescope has
detected the largest amount of gamma-rays to date, in the 20MeV 300GeV energy
range, allowing to perform a very sensitive indirect experimental search for DM
(by means of high-energy gamma-rays). DM forms large gravitationally bounded
structures, the halos, which can host entire galaxies, such as the Milky Way.
The DM distribution in the central part of the halos is not experimentally
know, despite a very large density enhancement might be present. As secondary
gamma rays production is very sensitive to WIMP density, a very effective
search can be performed from the regions where the largest density is expected.
Therefore the information provided by the DM halo N-body simulations are
crucial. The largest gamma-ray signal from DM annihilation is expected from the
centre of the Galaxy. In the same region a large gamma-ray background is
produced by bright discrete sources and the cosmic-rays interacting with the
interstellar gas and the photons fields.
Here we report an update of the indirect search for DM from the Galactic
Center (GC).Comment: 6 pages, 2 figures. Invited talk presented at the Workshop "SciNeGHE
2010", September 8-10, 2010, Trieste, Italy. To appear in Il Nuovo Cimento C
- Colloquia on physic
WIMP Gamma Rays From the Galactic Center with GLAST and Accelerator Comparison
We will describe the prospects for detecting gamma-rays from WIMP's
annihilation in the Galactic Center and we compare this search with the
possibilities at LHC and with space antimatter experiments like PAMELA.Comment: 3 pages, 6 figure
WIMP Gamma Rays From the Galactic Center with GLAST and Accelerator Comparison
We will describe the prospects for detecting gamma-rays from WIMP's
annihilation in the Galactic Center and we compare this search with the
possibilities at LHC and with space antimatter experiments like PAMELA.Comment: 3 pages, 6 figure
Bulges and disks in the local Universe. Linking the galaxy structure to star formation activity
We use a sample built on the SDSS DR7 catalogue and the bulge-disc
decomposition of Simard et al. (2011) to study how the bulge and disc
components contribute to the parent galaxy's star formation activity, by
determining its position in the star formation rate (SFR) - stellar mass
(M) plane at 0.020.1. We use the bulge and disc colours as proxy
for their SFRs. We study the mean galaxy bulge-total mass ratio (B/T) as a
function of the residual from the MS () and find that the
B/T- relation exhibits a parabola-like shape with the peak of the
MS corresponding to the lowest B/Ts at any stellar mass. The lower and upper
envelop of the MS are populated by galaxies with similar B/T, velocity
dispersion and concentration () values. Bulges above the MS are
characterised by blue colours or, when red, by a high level of dust
obscuration, thus indicating that in both cases they are actively star forming.
When on the MS or below it, bulges are mostly red and dead. At stellar masses
above M, bulges on the MS or in the green valley tend to
be significantly redder than their counterparts in the quiescence region,
despite similar levels of dust obscuration. The disc color anti-correlates at
any mass with the distance from the MS, getting redder when approaching the MS
lower envelope and the quiescence region. We conclude that the position of a
galaxy in the LogSFR-LogM plane depends on the star formation
activity of its components: above the MS both bulge and disk are actively star
forming. The nuclear activity is the first to be suppressed, moving the
galaxies on the MS. Once the disk stops forming stars as well, the galaxy moves
below the MS and eventually to the quiescence region. This is confirmed by a
large fraction () of passive galaxies with a secure two component
morphology.Comment: Version modified after referee comment
The quest for dark matter in dwarf spheroidal galaxies with the Cherenkov Telescope Array
Dwarf spheroidal galaxies are among the best environments that can be studied
with Cherenkov telescopes for indirect searches of -ray signals coming
from dark matter self-interaction (annihilation or decay), due to their
proximity and negligible background emission. We present new determinations of
the dark-matter amount - i.e. the astrophysical factors and - in
dwarf-galaxy halos obtained through the MCMC Jeans analysis of their brightness
and kinematic data. Such factors are of great importance to test the
performances of the next-generation -ray instruments such as the
Cherenkov Telescope Array in detecting dark-matter signals from astronomical
environments, or constraining the limits to dark-matter physics parameters
(particle mass and lifetime, annihilation cross section).Comment: 4 pages, 2 figures, 1 table, proceedings of the "RICAP-18 - 7th Roma
International Conference on Astroparticle Physics" held on 2018 Sep 04-07 at
Universit\`a di "Roma Tre", Via V. Volterra 62, I-00182 Roma, Italy (to
appear on EPJ Web of Conferences
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